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Journal articles on the topic 'Solar neutrino problem'

Author: Grafiati

Published: 4 June 2021

Last updated: 27 April 2022

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1

KWONG, WAIKWOK, and S. P. ROSEN. "THE SOLAR NEUTRINO PROBLEM AND BOUNDS ON SOLAR NEUTRINO FLUXES." Modern Physics Letters A 10, no. 19 (June 21, 1995): 1331–49. http://dx.doi.org/10.1142/s0217732395001460.

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We review the current status of the solar neutrino problem. A survey of the experiments and their results are given, and solar physics crucial to the understanding of these results are discussed. Semi-empirical methods are used to derive bounds on the fluxes of the three most important components (pp, 7Be and 8B) of the solar neutrino spectrum. The 8B neutrinos are directly measured to be about half of the theoretical prediction. Relative to their theoretical predictions, we find the 7Be neutrinos to be highly suppressed and the pp neutrinos not suppressed. We are also able to derive a lower bound on the pp flux.

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2

PAL, PALASH B. "PARTICLE PHYSICS CONFRONTS THE SOLAR NEUTRINO PROBLEM." International Journal of Modern Physics A 07, no. 22 (September 10, 1992): 5387–459. http://dx.doi.org/10.1142/s0217751x92002465.

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This review has four parts. In Part I, we describe the reactions that produce neutrinos in the sun and the expected flux of those neutrinos on the earth. We then discuss the detection of these neutrinos, and how the results obtained differ from the theoretical expectations, leading to what is known as the solar neutrino problem. In Part II, we show how neutrino oscillations can provide a solution to the solar neutrino problem. This includes vacuum oscillations, as well as matter enhanced oscillations. In Part III, we discuss the possibility of time variation of the neutrino flux and how a magnetic moment of the neutrino can explain the phenomenon. We also discuss particle physics models which can give rise to the required values of magnetic moments. In Part IV, we present some concluding remarks and outlook for the near future.

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3

Hargrove, C. K., and D. J. Paterson. "Solar-neutrino neutral-current detection methods in the Sudbury neutrino observatory." Canadian Journal of Physics 69, no. 11 (November 1, 1991): 1309–16. http://dx.doi.org/10.1139/p91-196.

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The Sudbury Neutrino Observatory will study the solar-neutrino problem through the detection of charged-current (CC), neutral-current (NC), and elastic-scattering (ES) interactions of solar neutrinos with heavy water. The measurement of the NC rate relative to the CC rate provides a nearly model-independent method of observing neutrino oscillations. The NC interaction breaks up the deuteron producing a neutron and a proton. The interaction rate in the original design is measured by observing Čerenkov light from showers produced by neutron-capture γ rays from the capture of the NC neutrons by a selected additive to the heavy water. These signals overlap the CC and ES signals, so that the measurement of the NC rate requires the subtraction of two signals obtained at different times. This paper describes our investigation of an alternate detection method in which the thermalized neutrons are captured by (n, α) or (n, p) reactions on light nuclei. The resulting charged-particle products are uniquely detected by scintillators or proportional counters, completely separating this NC signal from the CC and ES Čerenkov signals, thus simplifying its measurement, improving its significance, and allowing observation of otherwise unobservable short-term NC fluctuations. Although background rates for the new techniques have not yet been determined, the experimental advantages justify further development work.

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4

Spiro, M., and D. Vignaud. "Solar Neutrino Projects." International Astronomical Union Colloquium 121 (1990): 157–69. http://dx.doi.org/10.1017/s0252921100067919.

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AbstractAn overview of the solar neutrino projects is given, with an emphasis on the complementarity of the different experiments (gallium, indium, heavy water,...) to solve the solar neutrino problem that was raised by the chlorine and the Kamiokande results. The separation of the different sources of neutrinos in the Sun would contribute significantly to the astrophysical understanding of the Sun. Some of the planned experiments could be able to pinpoint neutrino oscillations (within a wide range of parameters) almost independently of solar models. Projects which are particularly sensitive to a variation of the neutrino flux with time are also discussed.

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5

Haxton, W. C. "The Solar Neutrino Problem." Annual Review of Astronomy and Astrophysics 33, no. 1 (September 1995): 459–503. http://dx.doi.org/10.1146/annurev.aa.33.090195.002331.

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6

Bahcall, John N. "The Solar-Neutrino Problem." Scientific American 262, no. 5 (May 1990): 54–61. http://dx.doi.org/10.1038/scientificamerican0590-54.

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7

Hampel, Wolfgang. "A solar neutrino problem?" Physics World 3, no. 9 (September 1990): 20–21. http://dx.doi.org/10.1088/2058-7058/3/9/18.

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8

Konijn, J. "The solar neutrino problem." European Journal of Physics 20, no. 6 (November 1, 1999): 399–407. http://dx.doi.org/10.1088/0143-0807/20/6/305.

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9

Prosper, Harrison B. "The solar neutrino problem." Pramana 54, no. 4 (April 2000): 611–22. http://dx.doi.org/10.1007/s12043-000-0154-6.

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10

de Sabbata, V., and C. Sivaram. "The solar-neutrino problem." Il Nuovo Cimento A 104, no. 10 (October 1991): 1577–79. http://dx.doi.org/10.1007/bf02817440.

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11

Bahcall, John N. "The solar neutrino problem." Solar Physics 100, no. 1-2 (October 1985): 53–63. http://dx.doi.org/10.1007/bf00158421.

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12

Zatsepin, G. T. "The solar neutrino problem." Nuclear Physics B - Proceedings Supplements 33, no. 1-2 (May 1993): 136–40. http://dx.doi.org/10.1016/0920-5632(93)90086-l.

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13

DEV, S., and JYOTI DHAR SHARMA. "THE STATUS OF THE SOLAR NEUTRINO PROBLEM IN THE RESONANT SPIN-FLAVOR PRECESSION SCENARIO WITH TWISTING SOLAR MAGNETIC FIELDS." Modern Physics Letters A 15, no. 22n23 (July 30, 2000): 1445–60. http://dx.doi.org/10.1142/s0217732300001870.

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Resonant spin-flavor precession scenario with twisting solar magnetic fields has been confronted with the solar neutrino data from various ongoing experiments. In particular, the anticorrelation apparent in the Homestake solar neutrino data has been taken seriously to constrain the twisting profiles of the magnetic field in the convective zone of the Sun. The twisting profiles, thus derived, have been used to calculate the neutrino detection rates for the Homestake, Kamiokande (super-Kamiokande) and the gallium experiments. It is found that the presence of twisting reduces the degree of anticorrelation in all the solar neutrino experiments. However, the anticorrelation in the Homestake experiment is expected to be more pronounced. Moreover, the anticorrelation of solar neutrino flux emerging from the southern solar hemisphere is expected to be stronger than that for the neutrinos emerging from the northern solar hemisphere.

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14

MORRISON, DOUGLAS R. O. "UPDATED REVIEW OF SOLAR MODELS AND SOLAR NEUTRINO EXPERIMENTS." International Journal of Modern Physics D 01, no. 02 (January 1992): 281–302. http://dx.doi.org/10.1142/s0218271892000148.

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The Conventional Wisdom that there is a Solar Neutrino Problem and that New Physics is required, is examined. The various solar evolutionary models, (or SSM), are described and in particular the four new 1992 papers. While the evolutionary models are generally robust, there are important assumptions and uncertainties (screening, nuclear reaction rates, etc.) which mean that the errors cannot be small. Diffusion in the Sun is expected to be significant but so far there is no calculation which includes all types of diffusion, especially turbulent diffusion. The new and important helioseismological results are shown to to be in agreement with some of the SSM calculations. The experimental results are beginning to be not inconsistent with the SSM calculations. Kamiokande is consistent with SSM calculations except for one with rather small errors. The new GALLEX result is in agreement with all SSM calculations within 1.3 to 2 standard deviations. The 1990 SAGE I experiment is shown to have no evidence of solar neutrinos and is inconsistent with all SSM calculations and with GALLEX. However the new 1991 SAGE II experiment finds neutrino rates not inconsistent with SSM calculations. The Chlorine experiment is significantly below SSM calculations and is inconsistent with Kamiokande. In particular the Chlorine claim that there is a variation of the solar neutrino flux with the inverse of the sunspot activity, which shows a correlation of five standard deviation significance, is in contradiction with the results of the Kamiokande experiment which finds no variation of the solar neutrino flux with time. The overall conclusion is that there is no compelling evidence for a Solar Neutrino Problem or need for New Physics. However the neutrinos could still have masses and further experiments with higher statistics are essential as they are one of the rare ways of studying this low mass region. Thus the Solar Neutrino Problem is becoming a Neutrino Mass Quest.

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15

Morrison, Douglas R. O. "Brief Review of Solar Models and Solar Neutrino Experiments." International Astronomical Union Colloquium 137 (1993): 100–107. http://dx.doi.org/10.1017/s0252921100017589.

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AbstractSolar Evolutionary Models are briefly reviewed and while the models are robust, there are uncertainties in the input data which justify rather larger errors. The 1992 experimental results from GALLEX, SAGE II and Kamiokande are shown to be consistent with calculated fluxes of solar neutrinos whereas the Chlorine results continue to be significantly low though this experiment has a problem with the high variability with time of its results in contradiction to Kamiokande. It is concluded that the evidence for a solar neutrino problem is not compelling and New Physics are not demanded. Further experiments are essential to search for neutrino masses and to study the Sun.

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16

SIMANJUNTAK, HERBERT P., and ANTO SULAKSONO. "ENERGY LOSSES OF SOLAR NEUTRINOS." Modern Physics Letters A 09, no. 24 (August 10, 1994): 2179–88. http://dx.doi.org/10.1142/s0217732394002033.

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The energy losses of solar neutrinos are calculated for weak and electromagnetic interactions with electrons. The effects of neutrino mass and oscillations are included in the calculations and we use the full energy dependence of the stopping power of matter for the total losses of energy. The full energy dependence shows that the energy losses are too small to explain the solar neutrino problem even with the use of Majorana neutrinos or interactions with protons.

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17

Kuo, T. K., and James Pantaleone. "Solar-Neutrino Problem and Three-Neutrino Oscillations." Physical Review Letters 57, no. 14 (October 6, 1986): 1805–8. http://dx.doi.org/10.1103/physrevlett.57.1805.

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18

Dar, A., A. Mann, Y. Melina, and D. Zajfman. "Neutrino oscillations and the solar-neutrino problem." Physical Review D 35, no. 12 (June 15, 1987): 3607–20. http://dx.doi.org/10.1103/physrevd.35.3607.

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19

Bitsch, M. E. Berbenni, and A. Vancura. "Neutrino oscillations and the solar neutrino problem." European Journal of Physics 10, no. 4 (October 1, 1989): 243–53. http://dx.doi.org/10.1088/0143-0807/10/4/001.

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20

MIRAMONTI, LINO, and VITO ANTONELLI. "ADVANCEMENTS IN SOLAR NEUTRINO PHYSICS." International Journal of Modern Physics E 22, no. 05 (May 2013): 1330009. http://dx.doi.org/10.1142/s0218301313300099.

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We review the results of solar neutrino physics, with particular attention to the data obtained and the analyses performed in the last decades, which were determinant to solve the solar neutrino problem (SNP), proving that neutrinos are massive and oscillating particles and contributing to refine the solar models. We also discuss the perspectives of the presently running experiments in this sector and of the ones planned for the near future and the impact they can have on elementary particle physics and astrophysics.

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21

Minakata, Hisakazu, and Hiroshi Nunokawa. "Pseudo Dirac neutrinos and the solar-neutrino problem." Physical Review D 45, no. 10 (May 15, 1992): R3316—R3320. http://dx.doi.org/10.1103/physrevd.45.r3316.

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22

INOUE, K. "REACTOR NEUTRINO EXPERIMENTS." International Journal of Modern Physics A 19, no. 08 (March 30, 2004): 1157–66. http://dx.doi.org/10.1142/s0217751x04019081.

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Previous searches for neutrino oscillations with reactor neutrinos have been done only with baselines less than 1 km. The observed neutrino flux was consistent with the expectation and only excluded regions were drawn on the neutrino-oscillation-parameter space. Thus, those experiments played important roles in understanding neutrinos from fission reactors. Based on the knowledge from those experiments, an experiment with about a 180 km baseline became possible. Results obtained from this baseline experiment showed evidence for reactor neutrino disappearance and finally provide a resolution for the long standing solar neutrino problem when combined with results from the solar neutrino experiments. Several possibilities to explore the last unmeasured mixing angle θ13 with reactor neutrinos have recently been proposed. They will provide complementary information to long baseline accelerator experiments when one tries to solve the degeneracy of oscillation parameters. Reactor neutrinos are also useful to study the neutrino magnetic moment and the most stringent limits from terrestrial experiments are obtained by measuring the elastic scattering cross section of reactor neutrinos.

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23

IGNATIEV, A. YU, and G. C. JOSHI. "THE CHARGED NEUTRINO: A NEW APPROACH TO THE SOLAR NEUTRINO PROBLEM." Modern Physics Letters A 09, no. 16 (May 30, 1994): 1479–88. http://dx.doi.org/10.1142/s0217732394001313.

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We have considered the effect of the reduction of the solar neutrino flux on earth due to the deflection of the charged neutrino by the magnetic field of the solar convective zone. The antisymmetry of this magnetic field about the plane of the solar equator induces the anisotropy of the solar neutrino flux thus creating the deficit of the neutrino flux on the earth. The deficit has been estimated in terms of solar and neutrino parameters and the condition of a 50% deficit has been obtained: Qν grad H≥10−18 eG/cm where Qν is the neutrino electric charge, grad H is the gradient of the solar toroidal magnetic field, e is the electron charge. Some attractive experimental consequences of this scenario are qualitatively discussed.

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24

Martinez, R., and S. F. Mantilla. "Mass problem in the Standard Model." EPJ Web of Conferences 182 (2018): 02084. http://dx.doi.org/10.1051/epjconf/201818202084.

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We propose a new SU(3)C ⊗ SU(2)L ⊗ U(1)Y ⊗ U(1)X gauge model which is non universal respect to the three fermion families of the Standard Model. We introduce additional one top-like quark, two bottom-like quarks and three right handed neutrinos in order to have an anomaly free theory. We also consider additional three right handed neutrinos which are singlets respect to the gauge symmetry of the model to implement see saw mechanism and give masses to the light neutrinos according to the neutrino oscillation phenomenology. In the context of this horizontal gauge symmetry we find mass ansatz for leptons and quarks. In particular, from the analysis of solar, atmospheric, reactor and accelerator neutrino oscillation experiments, we get the allow region for the Yukawa couplings for the charge and neutral lepton sectors according with the mass squared differences and mixing angles for the two neutrino hierarchy schemes, normal and inverted.

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25

Berezinsky, V. "The solar-neutrino problem, 1995." Il Nuovo Cimento C 18, no. 6 (November 1995): 671–84. http://dx.doi.org/10.1007/bf02506647.

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26

Wark, Dave. "Solar neutrino problem still perplexes." Physics World 5, no. 7 (July 1992): 20–21. http://dx.doi.org/10.1088/2058-7058/5/7/21.

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27

McDonald, Arthur B., Joshua R. Klein, and David L. Wark. "Solving the Solar Neutrino Problem." Scientific American 288, no. 4 (April 2003): 40–49. http://dx.doi.org/10.1038/scientificamerican0403-40.

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28

McDonald, Arthur B., Joshua R. Klein, and David L. Wark. "Solving the Solar Neutrino Problem." Scientific American Sp 15, no. 3 (January 2006): 22–31. http://dx.doi.org/10.1038/scientificamerican0206-22sp.

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29

Irani, Ardeshir. "Solving the Solar Neutrino Problem." Journal of High Energy Physics, Gravitation and Cosmology 07, no. 04 (2021): 1278–79. http://dx.doi.org/10.4236/jhepgc.2021.74077.

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30

OBERAUER, L. "LOW ENERGY NEUTRINO PHYSICS AFTER SNO AND KamLAND." Modern Physics Letters A 19, no. 05 (February 20, 2004): 337–48. http://dx.doi.org/10.1142/s0217732304013167.

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In the recent years important discoveries in the field of low energy neutrino physics (Eν in the ≈ MeV range) have been achieved. Results of the solar neutrino experiment SNO show clearly flavor transitions from νe to νμ,τ. In addition, the long standing solar neutrino problem is basically solved. With KamLAND, an experiment measuring neutrinos emitted from nuclear reactors at large distances, evidence for neutrino oscillations has been found. The values for the oscillation parameters, amplitude and phase, have been restricted. In this paper the potential of future projects in low energy neutrino physics is discussed. This encompasses future solar and reactor experiments as well as the direct search for neutrino masses. Finally the potential of a large liquid scintillator detector in an underground laboratory for supernova neutrino detection, solar neutrino detection, and the search for proton decay p→K+ν is discussed.

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31

BILENKY, S. M., C. GIUNTI, and C. W. KIM. "FINALLY NEUTRINO HAS MASS." International Journal of Modern Physics A 15, no. 05 (February 20, 2000): 625–50. http://dx.doi.org/10.1142/s0217751x00000318.

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The present status of the problem of neutrino mass, mixing and neutrino oscillations is briefly summarized. The evidence for oscillations of atmospheric neutrinos found recently in the Super-Kamiokande experiment is discussed. Indications in favor of neutrino oscillations obtained in solar neutrino experiments and in the accelerator LSND experiment are also considered. Implications of existing neutrino oscillation data for neutrino masses and mixing are discussed.

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32

Giunti, C., M. C. Gonzalez-Garcia, and C. Peña-Garay. "Four-neutrino oscillations and the solar neutrino problem." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 472, no. 3 (October 2001): 364–70. http://dx.doi.org/10.1016/s0168-9002(01)01273-6.

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33

MUGHAL, M. ANWAR, and K. AHMED. "NEUTRINO OSCILLATIONS AND FARADAY EFFECT." Modern Physics Letters A 09, no. 23 (July 30, 1994): 2097–106. http://dx.doi.org/10.1142/s0217732394001957.

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In analogy with the classical Faraday effect for the electromagnetic wave, a Faraday effect for massive neutrinos is found to be somewhat generic description of neutrino oscillations when neutrinos traverse a dense medium with or without a magnetic field. It is found that the Faraday angle for solar neutrino problem as an illustration of the Faraday effect for a neutrino wave provides conceptually convenient parametrization of the various oscillations scenarios.

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34

Hykawy, J. G. "Can photoionization effects explain the solar-neutrino problem?" Canadian Journal of Physics 73, no. 1-2 (January 1, 1995): 53–58. http://dx.doi.org/10.1139/p95-009.

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In a simple accretion model of the Sun, the inclusion of photoionizationlike phenomena leads to a set of initial conditions for solar burning that mimic a combination of the classic low-Z and high-Y models. When such initial conditions are used as input to the standard SunEV code, the predicted neutrino fluxes are in good agreement with those presently being observed in the Kamiokande, SAGE and GALLEX experiments. No new physics is required. It is possible that the combination of a low-Z and high-Y model, which is able to explain the solar neutrino deficit, might also provide good agreement with the presently observed helioseismic data. If data from the planned next generation of solar-neutrino experiments (e.g., SNO, SuperKamiokande) shows that the Mikheyer–Smirnov–Wolfenstein effect is not the solution to the solar-neutrino problem, experiments measuring the low-energy solar neutrino flux might show that a low-Z, high-Y combination model is valid.

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35

Spergel, David. "The Missing Mass and the Solar Neutrino Problem." Symposium - International Astronomical Union 117 (1987): 496. http://dx.doi.org/10.1017/s0074180900150752.

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If the halo of our galaxy is composed of weakly interacting particles, they will be captured by the sun. If the mass of these particles exceed 5 proton masses, they will remain in the Sun where they will serve as an effective means of transporting energy in the solar core. They will make the Sun's core more nearly isothermal, thus decreasing the rate of the PPIII reaction. If the halo is composed of particles with masses between 5 and 10 GeV and cross section between 10−34 and 10−37 cm2, this mechanism could resolve the solar neutrino problem. If these particles exist, they could be detected by a low temperature detector. However, if the particles annihilate in the Sun, (e.g. Photinos or Scalar Neutrinos), their number density will be too low.

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36

GRIMUS, W., and T. SCHARNAGL. "NEUTRINO PROPAGATION IN MATTER AND ELECTROMAGNETIC FIELDS." Modern Physics Letters A 08, no. 21 (July 10, 1993): 1943–59. http://dx.doi.org/10.1142/s0217732393001665.

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The neutrino propagation equations employed for possible solutions of the solar neutrino problem are reviewed and their derivation with the help of a Foldy-Wouthuysen transformation is discussed. The difference in the treatment of Dirac and Majorana neutrinos is particularly emphasized.

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37

RAJPOOT, SUBHASH. "A MODEL FOR SIMPSON’S 17 keV NEUTRINO." International Journal of Modern Physics A 07, no. 18 (July 20, 1992): 4441–48. http://dx.doi.org/10.1142/s0217751x92001988.

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Recent studies of β-decay spectra seem to confirm Simpson’s earlier findings that the electron neutrinos contain a small (1%) admixture of a 17 keV Dirac neutrino. An unconventional model with SU(2)L×SU(2)R×U(1)B−1 gauge interactions is presented in which all neutrinos are Dirac particles. Electron and muon neutrinos acquire seesaw Dirac masses of order 10−3eV for the MSW solution for the solar neutrino problem. The τ neutrino is identified as Simpson’s 17 keV neutrino. Constraints coming from cosmology and particle physics are shown to be satisfied.

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38

Antia, H. M., and S. M. Chitre. "Helioseismology and the Solar Neutrino Problem." Symposium - International Astronomical Union 185 (1998): 41–42. http://dx.doi.org/10.1017/s0074180900238229.

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The precisely measured frequencies of solar oscillations provide us with a unique tool to probe the solar interior with sufficient accuracy. These frequencies are principally determined by the dynamical quantities like sound speed, density or the adiabatic index of the solar material and a primary inversion of the observed frequencies yields the sound speed and density profiles inside the Sun (Gough et al. 1996). The equations of thermal equilibrium enable us to determine the temperature and chemical composition profiles, but for this additional prescriptions regarding the input physics (i.e., opacities, equation of state and nuclear energy generation rate) are required (Shibahashi 1993; Antia & Chitre 1995; Shibahashi & Takata 1996; Kosovichev 1996). This information in turn can be used to calculate the neutrino fluxes, and the seismic models can thus be used to explore the possibility of an astrophysical solution to the solar neutrino problem (Roxburgh 1996; Antia & Chitre 1997).

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39

Takata, M., and H. Shibahashi. "Seismic Solar Models and the Neutrino Problem." Symposium - International Astronomical Union 185 (1998): 21–24. http://dx.doi.org/10.1017/s0074180900238199.

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We determine the structure of the solar radiative zone with the imposition of the sound speed profile and the depth of the convection zone obtained from helioseismic analysis. We discuss the neutrino fluxes and capture rates using the resultant seismic solar model. We find that the seismic solar model cannot resolve the solar neutrino problem. The hydrogen and helium profiles of the Sun are obtained as a part of the solutions. We find that hydrogen is reduced in the core as expected in the theory of stellar evolution.

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40

Choudhury, Debajyoti, Raj Gandhi, J. A. Gracey, and Biswarup Mukhopadhyaya. "Two-loop neutrino masses and the solar neutrino problem." Physical Review D 50, no. 5 (September 1, 1994): 3468–76. http://dx.doi.org/10.1103/physrevd.50.3468.

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41

Pulido, João. "The solar neutrino problem and the neutrino magnetic moment." Physics Reports 211, no. 4 (February 1992): 167–99. http://dx.doi.org/10.1016/0370-1573(92)90071-7.

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42

Berezinsky, V. "Oscillation solutions to solar neutrino problem." Nuclear Physics B - Proceedings Supplements 80, no. 1-3 (January 2000): 17–32. http://dx.doi.org/10.1016/s0920-5632(99)00826-9.

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43

Dar, Arnon, and Giora Shaviv. "The solar neutrino problem – an update." Physics Reports 311, no. 3-5 (April 1999): 115–41. http://dx.doi.org/10.1016/s0370-1573(98)00094-5.

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44

Krastev, P. "Solutions to the solar neutrino problem." Nuclear Physics B - Proceedings Supplements 100, no. 1-3 (May 2001): 83–86. http://dx.doi.org/10.1016/s0920-5632(01)01417-7.

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45

Fangxiao, Dong. "Solar Neutrino Problem in Seesaw Model." Communications in Theoretical Physics 30, no. 1 (July 30, 1998): 113–16. http://dx.doi.org/10.1088/0253-6102/30/1/113.

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46

Bahcall, John N., and H. A. Bethe. "Solution of the solar-neutrino problem." Physical Review Letters 65, no. 18 (October 29, 1990): 2233–35. http://dx.doi.org/10.1103/physrevlett.65.2233.

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47

Sienkiewicz, R., J. N. Bahcall, and B. Paczynski. "Mixing and the solar neutrino problem." Astrophysical Journal 349 (February 1990): 641. http://dx.doi.org/10.1086/168351.

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48

Mann, Alfred K. "Problem Exposed by Solar‐Neutrino Work." Physics Today 39, no. 6 (June 1986): 11–13. http://dx.doi.org/10.1063/1.2815029.

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49

Roulet, Esteban. "E6leptoquarks and the solar-neutrino problem." Physical Review D 44, no. 12 (December 15, 1991): 3971–73. http://dx.doi.org/10.1103/physrevd.44.3971.

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50

Esposito, Salvatore, and Nicola Tancredi. "Pontecorvo Neutrino–Antineutrino Oscillations: Theory and Experimental Limits." Modern Physics Letters A 12, no. 25 (August 20, 1997): 1829–38. http://dx.doi.org/10.1142/s0217732397001862.

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We study Pontecorvo neutrino–antineutrino oscillations both in vacuum and in matter within a field theoretic approach, showing that this phenomenon can occur only if neutrinos have a Dirac–Majorana mass term. We find that matter effects suppress these oscillations and cannot explain the solar neutrino problem. On the contrary, a vacuum neutrino–antineutrino oscillations solution to this problem exists. We analyze this solution and the available data from laboratory experiments giving stringent limits on νe and νμ Majorana masses.

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